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Published February 1, 2018 | Published + Submitted
Journal Article Open

KIC 8164262: a heartbeat star showing tidally induced pulsations with resonant locking


We present the analysis of KIC 8164262, a heartbeat star with a high-amplitude (∼1 mmag), tidally resonant pulsation (a mode in resonance with the orbit) at 229 times the orbital frequency and a plethora of tidally induced g-mode pulsations (modes excited by the orbit). The analysis combines Kepler light curves with follow-up spectroscopic data from the Keck telescope, KPNO (Kitt Peak National Observatory) 4-m Mayall telescope and the 2.7-m telescope at the McDonald observatory. We apply the binary modelling software, PHOEBE, to the Kepler light curve and radial velocity data to determine a detailed binary star model that includes the prominent pulsation and Doppler boosting, alongside the usual attributes of a binary star model (including tidal distortion and reflection). The results show that the system contains a slightly evolved F star with an M secondary companion in a highly eccentric orbit (e = 0.886). We use the results of the binary star model in a companion paper (Fuller) where we show that the prominent pulsation can be explained by a tidally excited oscillation mode held near resonance by a resonance locking mechanism.

Additional Information

© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 October 11. Received 2017 October 11; in original form 2017 June 14. Published: 13 October 2017. The authors express their sincere thanks to NASA and the Kepler team for the high quality Kepler data. The Kepler mission is funded by NASA's Science Mission Directorate. We thank the Planet Hunters for finding this object and Professor Dan Fabrycky for notifying us about it. This work was also supported by the STFC (Science and Technology Funding Council). KH, ST and JF acknowledge support through NASA K2 GO grant (11-KEPLER11-0056) and NASA ADAP grant (16-ADAP16-0201). AP and KH acknowledge support from the NSF (grant #1517460). JF acknowledges partial support from NSF under grant nos. AST-1205732, PHY-1125915 and through a Lee DuBridge Fellowship at Caltech. We would like to thank the RAS for providing grants which enabled KH's attendance to conferences and thus enabled the development of collaborations and the successful completion of this work. AP acknowledges support through NASA K2 GO grant (NASA 14-K2GO1_2-0057). We acknowledge the observations taken using the 4-m Mayall telescope, KPNO (NOAO 2011A-0022); the Keck telescope, Mauna Kea and the 2.7-m telescope at the McDonald Observatory. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.

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Published - stx2673.pdf

Submitted - 1706.05051.pdf


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